Systematic errors in measuring parameters of non-spinning compact binary coalescences with post-Newtonian templates
Systematic errors in measuring parameters of non-spinning compact binary coalescences with post-Newtonian templates
复制标题
使用后牛顿模板测量非旋转致密二元聚结参数的系统误差
DOI：
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发表时间：
2010
期刊：
影响因子：
--
通讯作者：
Ajith Parameswaran
中科院分区：
文献类型：
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作者：
S. Bose;Shaon Ghosh;Ajith Parameswaran
我们研究的天体物理影响的重力波形的不准确和不完整的建模从紧凑的二元聚结（CBCs）。我们这样做的匹配滤波现象的吸气合并振铃（IMR）信号与银行的吸气相位模板建模的3.5后牛顿泰勒T1近似。选择模板的理由有三个方面。(1)现象IMR信号的螺旋相位，这是一个完整的IMR信号的例子，是仿照相同的泰勒T1近似。(2)在低质量的限制，合并和衰荡阶段是远远短于inspiral阶段，误差应该趋于消失的小值，因此，提供了一个重要的检查我们的模拟数值方面。(3)由于质量比大于10的双黑洞信号还不为人所知，而且由于涉及中子星的CBCs的信号受到其状态方程知识的不确定性的影响，因此仍在使用螺旋模板来搜索这些信号。从我们的数值模拟的结果进行了比较，使用模板参数空间上的Fisher矩阵的系统误差的分析计算。我们发现，即使对于组分质量为m1 = 10 M和m2 = 40 M的双黑洞，信噪比（SNR）的损失也可以高达45%。此外，同一对的估计总质量可能会偏离20%。这两种情况对于一些更高质量的组合来说都更糟。即使是对称质量比η的估计，在这个例子中也有近20%的误差，在这里研究的质量范围内，误差可能超过50%。这些误差显著地支配它们的统计对应物（在标称SNR为10时）。然而，可以通过允许具有非物理值η的模板来减轻SNR的损失。
We study the astrophysical impact of inaccurate and incomplete modeling of the gravitational waveforms from compact binary coalescences (CBCs). We do so by the matched filtering of phenomenological inspiral-merger-ringdown (IMR) signals with a bank of inspiral-phase templates modeled on the 3.5 post-Newtonian TaylorT1 approximant. The rationale for the choice of the templates is threefold. (1) The inspiral phase of the phenomenological IMR signals, which are an example of complete IMR signals, is modeled on the same TaylorT1 approximant. (2) In the low-mass limit, where the merger and ringdown phases are much shorter than the inspiral phase, the errors should tend to vanishingly small values and, thus, provide an important check on the numerical aspects of our simulations. (3) Since the binary black hole signals are not yet known for mass ratios above ten and since signals from CBCs involving neutron stars are affected by uncertainties in the knowledge of their equation of state, inspiral templates are still in use in searches for those signals. The results from our numerical simulations are compared with analytical calculations of the systematic errors using the Fisher matrix on the template parameter space. We find that the loss in signal-to-noise ratio (SNR) can be as large as 45% even for binary black holes with component masses m1 = 10 M⊙ and m2 = 40 M⊙. Also the estimated total mass for the same pair can be off by as much as 20%. Both of these are worse for some higher mass combinations. Even the estimation of the symmetric mass ratio η suffers a nearly 20% error for this example and can be worse than 50% for the mass ranges studied here. These errors significantly dominate their statistical counterparts (at a nominal SNR of 10). It may, however, be possible to mitigate the loss in SNR by allowing for templates with unphysical values of η.
相对论中子星合并产生的引力波与微物理状态方程
影响因子：
8.6
作者：
R. Oechslin;H.-Th. Janka
通讯作者：
H.-Th. Janka